Table 1:

Photometric data for BK Peg and the comparison stars.

Object	Sp. Type	Ref.	V		b-y		m1		c1		N(uvby)			N()
BK Peg	F8a	C10	9.982	7	0.362	6	0.143	12	0.456	12	176	2.639	7	9
		C10	10.463	4	0.369	7	0.136	11	0.477	4	6
HD 222249	F5 IVb	C10	7.146	6	0.309	4	0.177	8	0.503	8	118	2.645	3	8
		O83	7.139	5	0.317	3	0.158	4	0.503	4	1
		O94	7.151	9	0.317	3	0.161	3	0.507	2	3	2.645	8	3
		P69	7.010		0.303		0.190		0.487		2
HD 222391	G0 IIIc	C10	7.566	6	0.362	6	0.185	11	0.424	8	134	2.617	4	8
		O83	7.559	5	0.371	3	0.170	4	0.420	5	1
		O94			0.372	3	0.167	4	0.427	6	1	2.620	6	2
HD 223323	F2 IV-Vd	C10	7.084	6	0.290	5	0.138	10	0.414	9	189	2.636	7	13
		J96	7.076	4	0.302	1	0.123	1	0.407	1	9	2.640
		J96	7.094	2	0.300	0	0.128	5	0.409	4	2
		J96	7.089	1	0.299	0	0.120	0	0.406	1	2
		O83	7.080	6	0.296	5	0.124	5	0.412	4	4	2.643	5	4

References. ^(a) Popper (1983) ^(b) Harlan & Taylor (1970); ^(c) Heard (1956); ^(d) Harlan (1969).

Notes. C10 = This paper. J96 = Jordi et al. (1996). O83 = Olsen (1983). O94 = Olsen (1994). P69 = Perry (1969). For BK Peg, the information by C10 is the mean value outside eclipses (first line) and during the central part of secondary eclipse (second line), where 98% (y) of the light of the secondary component is eclipsed. N is the total number of observations used to form the mean values, and is the rms error (per observation) in mmag.